Propagation of Axial and Polar Gravitational Waves in Kantowski-Sachs Universe

TL;DR

This paper studies axial and polar gravitational waves in a Kantowski-Sachs universe using the Regge-Wheeler formalism, deriving solutions in vacuum and analyzing their properties, including damping effects and observational constraints.

Contribution

It provides analytical solutions for gravitational wave perturbations in Kantowski-Sachs spacetime and explores their physical implications and observational constraints.

Findings

Axial waves are damped due to anisotropy.

Polar waves can perturb matter fields and have frequencies 1000-2000 Hz.

Constraints on perturbation parameters are derived from GW data.

Abstract

We apply the Regge-Wheeler formalism to study axial and polar gravitational waves in Kantowski-Sachs universe. The background field equations and the linearised perturbation equations for the modes are derived in presence of matter. To find analytical solutions, we analyze the propagation of waves in vacuum spacetime. The background field equations in absence of matter are solved by assuming the expansion scalar to be proportional to the shear scalar. Using the method of separation of variables, the axial perturbation parameter $ h_0(t, r) $ is obtained from its wave equation. The other perturbation $ h_1(t, r) $ is then determined from $ h_0(t, r) $. The anisotropy of the background spacetime is responsible for the damping of the axial waves. The polar perturbation equations are much more involved compared to their FLRW counterparts, as well as to the axial perturbations in Kantowski-Sachs background. In both the axial and polar cases, the radial and temporal solutions separate out as products. The temporal part of the polar perturbation solutions are plotted against time to obtain an order of magnitude estimate of the frequency of the propagating GWs and lies in the range 1000-2000 Hz. Using standard observational data for the GW strain we have placed constraints on the parameters in the polar perturbation solutions. The perturbation equations in presence of matter show that the axial waves can cause perturbations only in the azimuthal velocity of the fluid without deforming the matter field. But the polar waves must perturb the energy density, the pressure and also the non-azimuthal components of the fluid velocity.